This quick-look data pool data set contains selected physical parameters computed centrally for each instrument at resolutions between one and five minutes, using quick-look, PI-provided algorithms. It was created in binary IBM 360 representation with unblocked, 3240-byte records. The first record of each file is a data pool file label containing satellite ID number; year, day of year, and seconds of day for the start and end of file; spacecraft clock; telemetry group number; minimum and maximum value of spin period found in this file; shadow times; and bit rate. The label record is followed by a number of data records containing day of year and seconds of day; s/c clock; bit rate; housekeeping and engineering items; spin period average; satellite position vector in GSE coordinates; and outputs of the investigators' quick-look data-processing algorithms for selected parameters from ten of the onboard experiments. The fast plasma data (Gosling/LANL) include four-level electron spectra, ion pseudondensities, average energies, and solar wind peak speeds and pseudodensities, at 5-minute resolution. The hot plasma (Frank, U. Iowa) algorithm outputs include proton densities, 10 keV electron fluxes, and energy range indicators, at 5-minute resolution. The fluxgate magnetometer data (Russell, UCLA) include 25 hourly parameters, plus the components of the magnetic field in spacecraft coordinates, at 1-minute resolution. The low-energy cosmic ray data (Hovestadt, MPI) include count rates of protons in three energy intervals between 0.17 and 20 MeV, plus those of alpha particles from 0.12 to 0.25 MeV and of Z>2 particles above 0.1 MeV, at 15-second resolution. The quasi-static electric field (Mozer, UCB) algorithm outputs indicate whether the experiment's electron guns were on or off during each 64-second interval. The plasma wave data (Gurnett, U. Iowa) include instantaneous samples from the 562 Hz filter channels of the electron and magnetic spectrum analysers, at 5-minute resolution. The plasma density data (Harvey, CESR) include indicators of the activity of the sounder and the propagation transmitters during each 64-second period. The energetic electron and proton algorithm outputs (Williams, APL) include both electron and proton differential fluxes in the 32 to 50 keV and the 80 to 126 keV energy ranges. These fluxes are taken in or near the spin-normal (nominally ecliptic) plane, at 5-minute resolution. The electron and proton experiment (K.Anderson, UCB) algorithm outputs include both electron and proton fluxes in the energy range 8 to 200 keV, at 5-minute resolution. The ion composition data (Sharp, Lockheed) include the cold plasma density and flags indicating the presence of high ion temperatures and bulk flow in the plasma, at 5-minute resolution. The Pool Tape Documentation (GSFC document X-692-77-129) (B29494 in NSSDC's Publications database) includes brief descriptions of the instruments, sometimes quite detailed, and also descriptions of the quick-look algorithms, also sometimes quite detailed.

This data set consists of three-dimensional proton and electron distribution functions. The energy range is 1 eV to 45 keV or 215 eV to 45 keV, according to mode. Time resolution for full distributions is 128 sec or 512 sec, depending on telemetry bit rate. Eight latitude and 16 azimuth bins are used, spanning 180 deg and 360 deg. Spacecraft position information is included. Data are currently in VAX binary format. Data are for discrete intervals 11/01/1977-12/31/1980, 10/15/1982-12/27/1983, 03/01/1986-06/01/1986

This data set consists of a set of daily files
with GIF-formatted spectrograms displaying color coded ion flux levels
as functions of time and of energy level, in each of 4 look-direction
quadrants, over the energy range of ~150 eV/q to 45 keV/q. Also
displayed is a single omni-directional spectrogram for electrons
in the same energy range. ISEE position data is listed once every
every four hours across the time axis.

of GSE X and Y components of the electric field; spacecraft potential, wave power in three frequency bands (3-14 Hz, 14-80 Hz, 120-600 Hz), spacecraft position in GSM, and 3-sec magnetic field data from the UCLA magnetometer. Uncertainty in Ex is 1-2 mV/meter, and less in Ey. Data values are binary integers.

This is a family of data sets containing 1-min
resolution ISEE 1 magnetic field and plasma parameters, in GSE
and GSM coordinates, both at the location of the ISEE 1 spacecraft
and as propagated to the location (17,0,0) Re, GSE. Data taken when
the spacecraft was inside the Spreiter et al (1966) model bow shock
were excluded. Propagation was done by J. Weygand using software
provided by D. Weimer. The software determines normal directions
to assumed planar phase fronts using a modified minimum variance
analysis of 1-min magnetic field data, and propagates data using
these normals and the ISEE1-observed solar wind flow velocity.
Magnetic field data consist of three Cartesian components, while
plasma data consist of three Cartesian components of the flow
velocity vector plus proton density and temperature. Different
subdirectories hold data for unique combinations of field vs.
plasma parameters, GSE vs. GSM coordinates, and unpropagated vs.
propagated data. See the VMO interface for a more detailed
breakout.

This data set contains magnetic field component
and magnitude averages every minute, with components given in spacecraft,
GSE and GSM coordinates. Standard deviations in the averages are given,
as are differences between the averages and model field vectors.
Geocentric (GSE and GSM) spacecraft position information is given,
as is ISEE1-ISEE2 separation vector information. ISEE 1 spin vector
direction and ISEE 1 velocity vector information, relative to the
Earth and to ISEE 2, are given. Miscellaneous other parameters are
also given. Data are accessible as plots, lists and files from
CDAWeb, and as CDF files from CDAWeb's ftp area.

4-sec vector magnetic field values recorded by the NASA ISEE-1 satellite, in spacecraft coordinates (close to GSE), available from UCLA and CDAWeb value-added interfaces and, via ftp, in binary from UCLA and in CDF from CDAWeb. (This descriptor updated, 6/20110, by J.King, to reflect CDAWeb accessibilityand to insert CDAWeb parameter keys.)

'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks,
and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978.
The International Sun-Earth Explorer (ISEE) Program consisted of three satellites
intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2
were launched on October 22, 1977 into highly elliptical geocentric orbits. The
satellites passed through the magnetosphere and into the magnetosheath during each
orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a
'halo orbit' about the the libration point situated about 240 earth radii (Re)
upstream between the earth and the sun. Plasma passing this point arrives at the
Earth about one hour later where it may cause changes that can be observed by ISEE 1
and ISEE-2. These two spacecraft, separated by a variable distance and with similar
instrument complements, were intended to resolve the space-time ambiguity associated
with measurements by a single spacecraft on thin boundaries which may be in motion
such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S.
contributions to the International Magnetospheric Study. ISEE-2 was built and managed
by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo
orbit' to explore the earth's deep tail region through much of 1983 on its way to an
encounter with the comet Giacobini Zinner in September 1985.
ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma,
and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these
thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination
of wave characteristics over a broad frequency range, including high-frequency
resolution spectrum scans, simultaneous high-time resolution electric and magnetic
frequency spectrum measurements, wave normal and Poynting flux measurements, and
wide-band waveform measurements.
PWI sampled the environment using three electric dipole antennas with lengths of
215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil
antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns
of wire and a preamplifier for magnetic-field measurements. The experiment's main
electronics consisted of four main elements: 1) a narrow-band sweep frequency
receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal
analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These
elements could be electrically connected to the six antennas in various combinations
in flight. Data for this file originate with an electric antenna and were measured
via the Electric Spectrum Analyzer (ESA).
The PWI ESA was designed to provide high time resolution spectrum measurements for
resolving wave emissions that are bursty or of a nonlinear nature. The ESA was a
20-channel analyzer covering the range from 5.62 Hz to 311 kHz. It had a relatively
coarse frequency resolution, with four frequency channels per decade and bandwidths
of +/-15 percent up to 10 kHz and +/-7.5 percent for 10 kHz and above. The ESA was
nominally intended for electric field measurements, though 2.2 percent of all ESA
measurements were made using the Z-axis magnetic search coil. The ISEE spacecraft
collected two separate data products with the PWI ESA. 1) A full frequency range
20-channel spectra and 2) a single-channel, rapid-sample series. The 'E_series'
variable in this file provides ESA rapid-sample measurements. Full frequency range
20-channel spectra are provided in a companion file set.
The rapid-sample series data were collected at 8-times the data rate of the 20-channel
spectra, thus there are 32 samples per second in high rate telemetry mode and 4 per
second in low-rate mode. Regardless of the telemetry mode, every 16 seconds the
rapid sample channel is incremented until reaching the highest frequency band of the
ESA (311 kHz), where it rolls over to the 5th band (56.2 Hz). Only the upper 16
channels of the ESA were sampled in this manner. Altogether this provides a 16-channel
frequency sweep every 4 minutes and 16 seconds. Unlike the SFR data, the time to
preform a complete frequency sweep is not affected by the telemetry mode, though
the number of samples in a sweep does increase by a factor of 4. Given the slowly
changing nature of the frequency channel compared to the sampling time these data
are stored as a time series, with the current frequency relegated to a status variable.
Nonetheless, frequency-time spectrograms may be constructed from these measurements
if desired.
For a detailed description of the Plasma Wave Instrument, the reader is referred to
the IEEE Geoscience Electronics reference above. A common acronym for the plasma
waves instrument in older documentation is GUM, which stands for for Gurnett Mother.
Since this acronym is not easily recognizable by the space physics community and
since no official acronym is provided in the instrument paper, the more common
short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

This dataset contains dynamic spectrogram PNG plots of the ISEE-1/PWI Spectrum Analyzer data. Each plot spans 12 hours. The dataset consists of files from 0-12UT and 12-24UT. These data were obtained from the Ev long wire antenna in the spin plane and the Bz search coil along the spin axis.
Each image consists of two panels. The title above the upper panel is "ISEE-1 PWI Spectrum Analyzer Ev Antenna and Bz Search Coil". Each panel is a plot of the power spectral density of received signal (color scale) as a function of operating frequency (in a logarithmic scale on the vertical axis) and time (horizontal axis). The upper panel is a plot of Electric Spectral Density (SD) the lower plot is Magnetic SD. Beneath the time labels on the horizontal axis of the spectrograms are ephemeris data: position of the spacecraft in radial distance (Earth radii), geomagnetic latitude, magnetic local time, and McIlwain L-shell. Overlaid on the upper plot are traces of the electron cyclotron frequencies. At the bottom of the image is the date, day number and time range.
Located in the same directory are the daily ISEE-1 PWI Sweep Frequency Receiver (SFR) spectrograms.

'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks,
and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978.
The International Sun-Earth Explorer (ISEE) Program consisted of three satellites
intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2
were launched on October 22, 1977 into highly elliptical geocentric orbits. The
satellites passed through the magnetosphere and into the magnetosheath during each
orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a
'halo orbit' about the the libration point situated about 240 earth radii (Re)
upstream between the earth and the sun. Plasma passing this point arrives at the
Earth about one hour later where it may cause changes that can be observed by ISEE 1
and ISEE-2. These two spacecraft, separated by a variable distance and with similar
instrument complements, were intended to resolve the space-time ambiguity associated
with measurements by a single spacecraft on thin boundaries which may be in motion
such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S.
contributions to the International Magnetospheric Study. ISEE-2 was built and managed
by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo
orbit' to explore the earth's deep tail region through much of 1983 on its way to an
encounter with the comet Giacobini Zinner in September 1985.
ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma,
and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these
thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination
of wave characteristics over a broad frequency range, including high-frequency
resolution spectrum scans, simultaneous high-time resolution electric and magnetic
frequency spectrum measurements, wave normal and Poynting flux measurements, and
wide-band waveform measurements.
PWI sampled the environment using three electric dipole antennas with lengths of
215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil
antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns
of wire and a preamplifier for magnetic-field measurements. The experiment's main
electronics consisted of four main elements: 1) a narrow-band sweep frequency
receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal
analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These
elements could be electrically connected to the six antennas in various combinations
in flight. Data for this file originate with the spectrum analyzers.
The PWI Spectrum Analyzers were designed to provide high time resolution spectrum
measurements for resolving wave emissions that are bursty or of a nonlinear nature.
The pair consisted of a 20-channel analyzer covering the range from 5.62 Hz to
311 kHz, and a 14-channel analyzer covering the range from 5.62 Hz to 10 kHz.
These analyzers have a relatively coarse frequency resolution, with four frequency
channels per decade and bandwidths of +/-15 percent up to 10 kHz and +/-7.5 percent
for 10 kHz and above. The center frequencies and bandwidths of the 20- and 14-channel
analyzers are identical. The 20-channel analyzer was nominally intended for electric
field measurements (which extend up to higher frequencies than the magnetic
measurements), and the 14-channel analyzer was nominally intended for magnetic field
measurements. All channels are sampled simultaneously so that electric-to-magnetic
field ratios could be accurately determined.
For a detailed description of the Plasma Wave Instrument, the reader is referred to
the IEEE Geoscience Electronics reference above. A common acronym for the plasma
waves instrument in older documentation is GUM, which stands for for Gurnett Mother.
Since this acronym is not easily recognizable by the space physics community and
since no official acronym is provided in the instrument paper, the more common
short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

This dataset contains dynamic spectrogram PNG plots of the ISEE1/PWI Sweep Frequency Receiver (SFR) data. Each plot spans one day. These data were obtained from the Ev long wire antenna in the spin plane and the Eu two-sphere antenna via the SFR receiver.
The title above each spectrogram is "ISEE-1 PWI Sweep Frequency Receiver Ev and Eu Antennas". Each spectrogram is a plot of the power spectral density of received signal (color scale) as a function of operating frequency (in a logarithmic scale on the vertical axis) and time (horizontal axis). Beneath the time labels on the horizontal axis of the spectrograms are ephemeris data: position of the spacecraft in radial distance (Earth radii), geomagnetic latitude, magnetic local time, and McIlwain L-shell. Overlaid on each image are traces of the electron cyclotron frequencies.
Located in the same directory are are the 12 hour ISEE-1 PWI Spectrum Analyzer (SA) spectrograms.

'The ISEE-1 and -2 Plasma Wave Investigation' D. A. Gurnett, F. L. Scarf, R. W. Fredricks,
and E. J. Smith, IEEE Transactions on Geoscience Electronics, Vol. GE-16, p. 225-230, 1978.
The International Sun-Earth Explorer (ISEE) Program consisted of three satellites
intended to study the Earth's magnetosphere and the solar wind. ISEE-1 and ISEE-2
were launched on October 22, 1977 into highly elliptical geocentric orbits. The
satellites passed through the magnetosphere and into the magnetosheath during each
orbit. ISEE-3 was launched on August 12, 1978 and subsequently inserted into a
'halo orbit' about the the libration point situated about 240 earth radii (Re)
upstream between the earth and the sun. Plasma passing this point arrives at the
Earth about one hour later where it may cause changes that can be observed by ISEE 1
and ISEE-2. These two spacecraft, separated by a variable distance and with similar
instrument complements, were intended to resolve the space-time ambiguity associated
with measurements by a single spacecraft on thin boundaries which may be in motion
such as the bow shock and the magnetopause. ISEE-1 and ISEE-3 were the principal U. S.
contributions to the International Magnetospheric Study. ISEE-2 was built and managed
by the European Space Agency. In September 1982 ISEE-3 was diverted from its 'halo
orbit' to explore the earth's deep tail region through much of 1983 on its way to an
encounter with the comet Giacobini Zinner in September 1985.
ISEE-1 had a complement of thirteen experiments to measure the waves, fields, plasma,
and particles. The University of Iowa Plasma Wave Instrument (PWI) was one of these
thirteen. The ISEE-1 plasma waves instrument provided a comprehensive determination
of wave characteristics over a broad frequency range, including high-frequency
resolution spectrum scans, simultaneous high-time resolution electric and magnetic
frequency spectrum measurements, wave normal and Poynting flux measurements, and
wide-band waveform measurements.
PWI sampled the environment using three electric dipole antennas with lengths of
215, 73.5, and 0.61 meters for electric-field measurements, and a triaxial search coil
antenna with three 16-in high permeability mu-metal cores each wound with 10,000 turns
of wire and a preamplifier for magnetic-field measurements. The experiment's main
electronics consisted of four main elements: 1) a narrow-band sweep frequency
receiver, 2) a pair of high time resolution spectrum analyzers, 3) a wave normal
analyzer, and 4) an analog waveform receiver (also called a wide-band receiver). These
elements could be electrically connected to the six antennas in various combinations
in flight. Data for this file originate with an electric antenna and were measured
via the Sweep Frequency Receiver (SFR).
The narrow-band sweep frequency receiver was intended to provide very high
resolution spectrums with low time resolution for analyzing relatively steady narrow-
band emissions such as upper hybrid resonance noise, electron plasma oscillations, and
electron cyclotron harmonics. The receiver has 32 frequency steps in each of four
bands covering the frequency range from approximately 100 Hz to 400 kHz. The
frequency steps are logarithmically spaced with a frequency resolution of about 6.5
percent of the center frequency. The dynamic range of the receiver is 100 dB in the
lowest three frequency bands, and 80 dB in the highest. Because the time resolution
of the SFR is greater than the typical delay times for waves propagating between
the two spacecraft, this receiver is only included on ISEE-1.
For a detailed description of the Plasma Wave Instrument, the reader is referred to
the IEEE Geoscience Electronics reference above. A common acronym for the plasma
waves instrument in older documentation is GUM, which stands for for Gurnett Mother.
Since this acronym is not easily recognizable by the space physics community and
since no official acronym is provided in the instrument paper, the more common
short hand 'PWI' is used to refer to the Plasma Wave Instrument in this archive.

This data set, held in CDAWeb as ISEE1_H0_FE,
contains electron moments from the Vector Electron Spectrometer
(VES), and spacecraft position vectors, at 9s or 18s resolution,
depending on spacecraft telemetry rate. The data set
also holds 1-min averages of the measured magnetic field
vector. Electron moments include density, flow velocity,
temperature and its anisotropy, and heat flux vector. Also given
are the pressure tensor, its diagonalizing eigenvector, and the
angle between its principal axis and the ambient magnetic field
vector. These parameters are based on distributions accumulated
in 3 sec but telemetered over 9s or 18s. Ancillary information
given includes the spacecraft spin period, the spacecraft
potential, the energy channels above this potential on which the
moments for this record were based, and on/off flags for the
Harvey and Mozer experiments.

ISEE-1 Fast Plasma Experiment data linearly interpolated to have the measurements on the minute at 60 s resolution data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies and cross correlation studies on solar wind.

ISEE-1 Fast Plasma Experiment data linearly interpolated to have the measurements on the minute at 60 s resolution data in GSM coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies and cross correlation studies on solar wind.

ISEE-1 Fast Plasma Experiment Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution data in GSE coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ??Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,?? J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

ISEE-1 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution FPE data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ??Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,?? J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

ISEE-1 linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies and cross correlation studies on solar wind.

ISEE-1 linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSM coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies and cross correlation studies on solar wind.

ISEE-1 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSE coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies. References: Weimer, D. R. (2004), Correction to ??Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,?? J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

ISEE-1 Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution tri-axial fluxgate magnetometer data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ??Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,?? J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

ISEE-1 Weimer propagated solar wind data and linearly interpolated time delay, cosine angle, and goodness information of propagated data at 1 min Resolution. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to ??Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique,?? J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.